Great. SuperWASP is a true inventory of transiting hot Jupiters, better than Kepler or Corot. In a few years of further discoveries it could start to draw statistics on its own about characteristics of this particular class of planetary population.

We report the discovery by the WASP transit survey of a highly-irradiated, massive (2.258 +/- 0.072 MJup) planet which transits a bright (V = 10.6), evolved F8 star every 2.9 days. The planet, WASP-71b, is larger than Jupiter (1.50 +/- 0.11 RJup), but less dense (0.67 +/- 0.14 {\rho}Jup). We also report spectroscopic observations made during transit with the CORALIE spectrograph, which allow us to detect the Rossiter-McLaughlin effect. We determine the sky-projected angle between the stellar-spin and planetary-orbit axes to be {\lambda} = 19.8 +/- 9.9 degrees.

We report the discovery of a transiting planet with an orbital period of 1.36d orbiting the brighter component of the visual binary star BD -07 436. The host star, WASP-77A, is a moderately bright G8V star (V=10.3) with a metallicity close to solar ([Fe/H]= 0.0 +- 0.1). The companion star, WASP-77B, is a K-dwarf approximately 2 magnitudes fainter at a separation of approximately 3arcsec. The spectrum of WASP-77A shows emission in the cores of the Ca II H and K lines indicative of moderate chromospheric activity. The WASP lightcurves show photometric variability with a period of 15.3 days and an amplitude of about 0.3% that is probably due to the magnetic activity of the host star. We use an analysis of the combined photometric and spectroscopic data to derive the mass and radius of the planet (1.76+-0.06MJup, 1.21+-0.02RJup). The age of WASP-77A estimated from its rotation rate (~1 Gyr) agrees with the age estimated in a similar way for WASP-77B (~0.6 Gyr) but is in poor agreement with the age inferred by comparing its effective temperature and density to stellar models (~8 Gyr). Follow-up observations of WASP-77 Ab will make a useful contribution to our understanding of the influence of binarity and host star activity on the properties of hot Jupiters.

No TTVs for WASP-2. Seems to be a generic property of hot Jupiter systems, which means that the systems most easily observed from the ground are those which are least likely to exhibit TTV:

It is likely that the lack of TTVs being detected from the ground is due to a fundamental property of the systems that are being studied. The vast majority of ground–based follow–up is focused on hot–Jupiter systems, since resolving their transit depths is achievable even with modest aperture telescopes and non photometric observing conditions. However, as outlined by Steffen et al. (2012b), hot–Jupiter systems observed by Kepler also fail to show detectable TTVs, or any evidence for being in a multi–planet system. Their neighbors in exoplanet parameter space, loosely termed warm-Jupiters and hot–Neptunes, do show evidence for both TTVs and transiting companions. What this suggests is a unique dynamical pathway for the formation of contemporary hot–Jupiters, such as multi–planet scattering (e.g. Beaugé & Nesvorný 2012) leading to the ejection of lesser bodies from the system.

Oooh nice, looks like it might be a good target to follow-up for studying warm Jupiter atmospheres:

WASP-80b’s equilibrium temperature will be around 800K (for an albedo of 0.1). The planet-to-star contrast is favourable for future observation of the emission spectrum of the planet, because it is hosted by a star ~1500K colder than the usual targets. Furthermore, the near 3% depth of the transit makes this gas giant one of the most suitable targets for transmission spectroscopy.

We report the discovery of two transiting hot Jupiters, WASP-65b (M_pl = 1.55 +/- 0.16 M_J; R_pl = 1.11 +/- 0.06 R_J), and WASP-75b (M_pl = 1.07 +/- 0.05 M_J; R_pl = 1.27 +/- 0.05 R_J). They orbit their host star every 2.311, and 2.484 days, respectively. The planet host WASP-65 is a G6 star (T_eff = 5600 K, [Fe/H] = -0.07 +/- 0.07, age > 8 Gyr); WASP-75 is an F9 star (T_eff = 6100 K, [Fe/H] = 0.07 +/- 0.09, age of 3 Gyr). The mean density of WASP-65b is similar to that of Jupiter (rho_pl = 1.13 +/- 0.08 rho_J), and in fact, WASP-65b is one of the densest planets with a mass between 0.1 and 2.0 M_J, a mass range in which a large fraction of the known planets have been found to be inflated with respect to theoretical planet models. WASP-65b is one of only a handful of planets with masses of around 1.5 M_J, a mass regime surprisingly underrepresented among the currently known hot Jupiters. The radius of Jupiter-mass WASP-75b is slightly inflated (< 10%) as compared to theoretical planet models with no core, and has a density similar to that of Saturn (rho_pl = 0.52 +/- 0.06 rho_J).

We report the discovery of WASP-103b, a new ultra-short-period planet (P=22.2 hr) transiting a 12.1 V-magnitude F8-type main-sequence star (1.22+-0.04 Msun, 1.44-0.03+0.05 Rsun, Teff = 6110+-160 K). WASP-103b is significantly more massive (1.49+-0.09 Mjup) and larger (1.53-0.07+0.05 Rjup) than Jupiter. Its large size and extreme irradiation (around 9 10^9 erg/s/cm^2) make it an exquisite target for a thorough atmospheric characterization with existing facilities. Furthermore, its orbital distance is less than 20% larger than its Roche radius, meaning that it might be significantly distorted by tides and might experience mass loss through Roche-lobe overflow. It thus represents a new key object for understanding the last stage of the tidal evolution of hot Jupiters.

We report the discovery of the planets WASP-20b and WASP-28b along with measurements of their sky-projected orbital obliquities. WASP-20b is an inflated, Saturn-mass planet (0.31 MJup ; 1.46 RJup ) in a 4.9-day, near-aligned (λ=8.1±3.6°) orbit around CD-24 102 (V =10.7; F9). WASP-28b is an inflated, Jupiter-mass planet (0.91 MJup ; 1.21 RJup ) in a 3.4-day, near-aligned (λ=8±18°) orbit around a V =12, F8 star. As intermediate-mass planets in short orbits around aged, cool stars (7-1+2 Gyr for WASP-20 and 5-2+3 Gyr for WASP-28; both with T eff < 6250 K), their orbital alignment is consistent with the hypothesis that close-in giant planets are scattered into eccentric orbits with random alignments, which are then circularised and aligned with their stars' spins via tidal dissipation.

So what's going on with the discovery of WASP-28b? I take it then that the West et al. preprint that's been on the SuperWASP website since 2010 never got accepted in a refereed journal (was it ever submitted I wonder)?